Witnessing the birth of the red sequence: the physical scale and morphology of dust emission in hyper-luminous starbursts in the early Universe

We present high-spatial-resolution (∼0.12′′∼0.12″ or ≈800pc≈800pc at z=4.5𝑧=4.5) ALMA 870μ870𝜇m dust continuum observations of a sample of 44 ultrared dusty star-forming galaxies (DSFGs) selected from the H-ATLAS and HerMES far-infrared surveys because of their red colors from 250 to 500 μ𝜇m: S500/S250>1.5𝑆500/𝑆250>1.5 and S500/S350>1.0𝑆500/𝑆350>1.0. With photometric redshifts in the range z∼4𝑧∼4-6, our sample includes the most luminous starbursting systems in the early Universe known so far, with total obscured star-formation rates (SFRs) of up to ∼4,500M⊙yr−1∼4,500𝑀⊙yr−1, as well as a population of lensed, less intrinsically luminous sources. The lower limit on the number of ultrared DSFGs at 870 μ𝜇m (with flux densities measured from the ALMA maps and thus not affected by source confusion) derived in this work is in reasonable agreement with models of galaxy evolution, whereas there have been reports of conflicts at 500 μ𝜇m (where flux densities are derived from SPIRE). Ultrared DSFGs have a variety of morphologies (from relatively extended disks with smooth radial profiles, to compact sources, both isolated and interacting) and an average size, θFWHM𝜃FWHM, of 1.46±0.41kpc1.46±0.41kpc, considerably smaller than the values reported in previous work for less-luminous DSFGs at lower redshifts. The size and the estimated gas-depletion times of our sources are compatible with their being the progenitors of the most massive, compact, red-and-dead galaxies at z∼2𝑧∼2-3, and ultimately of local ultra-massive elliptical galaxies or massive galaxy clusters. We are witnessing the birth of the high-mass tail of the red sequence of galaxies.